Optimization Approach for the Computation of 3D Magnetohydrostatic Coronal Equilibria From Multi-Spacecraft Observations

Details Optimization Approach for the Computation of 3D Magnetohydrostatic Coronal Equilibria From Multi-Spacecraft Observations Optimization Approach for the Computation of 3D Magnetohydrostatic Coronal Equilibria From Multi-Spacecraft Observations

Dec 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007agufmsh14b..05n&link_type=abstract

American Geophysical Union, Fall Meeting 2007, abstract #SH14B-05

Astronomy and Astrophysics

Astrophysics

7500 Solar Physics, Astrophysics, And Astronomy, 7509 Corona, 7524 Magnetic Fields, 7529 Photosphere

Scientific paper

We cannot measure the 3D coronal magnetic field and plasma pressure/density distribution directly. To derive these quantities we propose a modelling approach based on observational data from multiple instruments. Our aim is to use measurements of the photospheric magnetic field vector (e.g. from Hinode/SOT and in future from SDO/HMI) and plasma images from two viewpoints -as provided by STEREO- as input for a newly developed magnetohydrostatic optimization code. The resulting 3D magnetic field and plasma distribution is a self-consistent equilibrium within the magnetohydrostatic approach. Here we test our code with the help of an exact magnetohydrostatic equilibrium and extracted synthetic observational data, which allow us to evaluate the accuracy of our method. We find that the method reconstructs the equilibrium accurately, with residual forces of the order of the discretisation error of the exact solution. The correlation with the reference solution is better than 99.9 percent and the magnetic energy is computed accurately with an error of less than 0.1 percent. We are planning to use this method with real observational data as input as soon as possible.

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